Solar System Physics I Dr Martin Hendry 5 lectures, beginning Autumn 2007 Department of Physics and Astronomy Astronomy 1X Session

Section 5: The Ideal Gas Law The atmospheres of planets (and the Sun too) can be modelled as an Ideal Gas – i.e. consisting of point-like particles (atoms or molecules) moving in random directions and interacting through perfectly elastic collisions.

Section 5: The Ideal Gas Law The atmospheres of planets (and the Sun too) can be modelled as an Ideal Gas – i.e. consisting of point-like particles (atoms or molecules) moving in random directions and interacting through perfectly elastic collisions. We assume that the atmosphere has an equation of state, which links its pressure, density and temperature: Volume of the gas Gas pressure, a measure of the force of the collisions Number of particles in the gas Boltzmann constant: Gas temperature, a measure of the K.E. of the particles degrees Kelvin (5.1)

We can also write eq. (5.1) in the form Here is the number density of gas particles. (5.2)

We can also write eq. (5.1) in the form Here is the number density of gas particles. Also we can write (5.2) (5.3) Mass density of the gas Average mass of a gas particle

We can also write eq. (5.1) in the form Here is the number density of gas particles. Also we can write So if we introduce Then, from eqs. (5.2) – (5.4) (5.2) (5.3) Mass density of the gas Average mass of a gas particle (5.4) Average mass of a gas particle in units of mass of hydrogen atom (5.5)

is the “mean square speed” of the gas particles Factor of 3 on the RHS comes from the 3 dimensions (“degrees of freedom”) in which the particles can move. The gas has energy of per degree of freedom The temperature of the gas is a measure of the average kinetic energy of the particles. Suppose all particles have mass. Then we define Note (5.6)

At a temperature of absolute zero, i.e., all gas motions cease. Gas pressure drops to zero. From eq. (5.5) Substituting from eqs. (5.2) and (5.3) (5.7) (5.8)

Section 6: Hydrostatic Equilibrium The pressure (and hence the density and temperature) is not constant throughout a planetary atmosphere. A balance is maintained between the outward pressure force and the inward gravitational force. We call this balance hydrostatic equilibrium. Let’s assume (as we did in section 2 for the interior of a planet) that the density of gas in the atmosphere is spherically symmetric. We can then derive an expression for how the pressure changes as a function of height in the planet’s atmosphere. (we do this using calculus, forming a differential equation)

Consider a small cylinder of gas in the planet’s atmosphere, the bottom of which is a distance from the centre of the planet. Let the area of the cylinder be and its height be. Suppose the cylinder contains a mass of gas. What forces will be exerted on this cylinder by the rest of the atmosphere?...

Consider a small cylinder of gas in the planet’s atmosphere, the bottom of which is a distance from the centre of the planet. Let the area of the cylinder be and its height be. Suppose the cylinder contains a mass of gas. What forces will be exerted on this cylinder by the rest of the atmosphere?... The horizontal forces on the walls of the cylinder will cancel out

Upper face: Downward force, due to pressure exerted by gas above the cylinder Notes: (1) we are taking upwards as positive (2) we are using here the relation pressure = force per unit area (6.1) * * There will also be a downward force due to the weight of atmosphere above the cylinder, but we don’t consider that here since it will also apply to the lower face.

Lower face: Upward force, due to pressure of the gas below the cylinder, and downward force, due to the weight of the gas in the cylinder. (6.2) Notes: (1) is the mass contained within radius from the planet’s centre (2) The gravitational force term in eq. 6.2 is an approximation, since the cylinder does not all lie at distance from the centre. This is OK provided

We can also write the mass of gas in the cylinder as density x volume: Substituting into eq. (6.3) gives To keep the cylinder static, we require that there be no net force on it, i.e. (6.4) (6.5) We can re-write eq. (6.2) as (6.3)

So Dividing by and re-arranging In the limit as the LHS is the derivative of with respect to i.e. the rate of change of pressure with radius. Finally,then, we have (6.6) (6.7) (6.8) Also referred to as the pressure gradient

Since the density and gravitational acceleration are both positive, this means that i.e. decreases with increasing radius. How fast?... We define the pressure scale height via If we make the assumption that is constant, then we can find an expression for the pressure as a function of radius. (6.9) (6.10)

Re-arranging eq. (6.10) This is a differential equation. We solve it by integrating both sides. (6.11) By assuming the scale height is constant, we can take it out of the integral

Re-arranging eq. (6.10) This is a differential equation. We solve it by integrating both sides. i.e. (6.11) By assuming the scale height is constant, we can take it out of the integral (6.12) Natural logarithm

Re-arranging eq. (6.10) This is a differential equation. We solve it by integrating both sides. i.e. The constant can be fixed by the pressure at, say (6.11) By assuming the scale height is constant, we can take it out of the integral (6.12) Natural logarithm (6.13)

Eq. (6.13) makes sense for e.g. the Sun, which is gaseous throughout. For a planet like the Earth, with a solid interior, we can write Radius of surface Height above surface

Eq. (6.13) makes sense for e.g. the Sun, which is gaseous throughout. For a planet like the Earth, with a solid interior, we can write We then fix the constant to be the pressure at the surface, The Earth’s surface pressure is defined as 1 atmosphere Radius of surface Height above surface (6.14)

From eqs. (6.8) and (6.10) For an ideal gas, from eq. (5.5) So (6.15)

From eqs. (6.8) and (6.10) For an ideal gas, from eq. (5.5) So As increases, so does, i.e. the atmosphere extends further. As increase, decreases. i.e. atmosphere less extended. (6.15)

From eqs. (6.8) and (6.10) For an ideal gas, from eq. (5.5) So As increases, so does, i.e. the atmosphere extends further. As increase, decreases. i.e. atmosphere less extended. Substituting in eq. (6.14) (6.15) (6.16)

The atoms or molecules in a planet’s atmosphere are constantly moving. If they are moving fast enough, they can escape. From eq. (3.7), this requires But the particles will have a distribution of speeds - some will exceed the escape speed, while others will not. When a sufficient fraction of the particles exceed the escape speed, the planet will effectively ‘lose’ its atmosphere. Section 7: Escape of a Planetary Atmosphere (7.1)

A good ‘rule of thumb’ is: A particular component of a planet’s atmosphere will be lost if, for that component, is the ‘root mean square’ speed, the square root of the mean square speed we met in Section 5. We can use the results of Section 5 to relate the escape criterion to temperature, using: (7.2) (7.3)

So a particle of mass will escape if We define the escape temperature The more massive the planet, the hotter it must be before a given atmospheric component is lost. (7.4) (7.5)